论文标题
模拟矮星系中的AGN淬灭
AGN quenching in simulated dwarf galaxies
论文作者
论文摘要
我们检查了$ 328 $隔离矮星系的淬火特性$ \ left（10^{8} <m _ {\ rm star}/m_ \ odot <10^{10} \ right <10^{10} \ right）$ in \ rom {} cesmologicalmologicalmologic necomological incomological holdymologic nocal ne使用模拟观察方法，我们识别出具有猝灭星形形成的孤立矮星系，并与NASA Sloan Atlas（NSA）中的淬灭分数进行直接比较。与其他宇宙学模拟类似，我们发现低于$ m _ {\ rm star} <10^{9} m_ \ odot $的淬火，孤立的矮星系群在NSA中未检测到。我们发现，\ rom {}中存在巨大的黑洞（MBHS）是对淬火，孤立的矮人的主要负责，而没有MBH的孤立矮人与在田间观察到的静态分数一致。淬火发生在$ z = 0.5-1 $之间，在此期间，MBH反馈加热或撤离了可用的星形气体供应。合并或互动似乎在触发MBH反馈方面没有任何作用。在低恒星质量下，$ m _ {\ rm star} \ Lessim 10^{9.3} m_ \ odot $，随着MBH在中央地区慢慢加热气体，Quenching逐渐跨越了几个GYR。在较高的恒星质量下，$ m _ {\ rm star} \ gtrsim 10^{9.3} m_ \ odot $，淬灭迅速发生在$ 1 $ gyr之内，MBH撤离气体从Galaxy的Central Vacuating Gas撤离了GALAXY的少数KPC，并驱动到Halo的郊区。我们的结果表明，在该场中矮星系中，通过MBH反馈抑制了大量恒星形成的可能性。另一方面，由于MBH引起的矮星系的明显过度淬火表明，矮人中MBH需要更高的分辨率和/或更好的建模，而淬灭的分数为限制电流模型提供了机会。
We examine the quenching characteristics of $328$ isolated dwarf galaxies $\left(10^{8} < M_{\rm star}/M_\odot < 10^{10} \right)$ within the \Rom{} cosmological hydrodynamic simulation. Using mock observation methods, we identify isolated dwarf galaxies with quenched star formation and make direct comparisons to the quenched fraction in the NASA Sloan Atlas (NSA). Similar to other cosmological simulations, we find a population of quenched, isolated dwarf galaxies below $M_{\rm star} < 10^{9} M_\odot$ not detected within the NSA. We find that the presence of massive black holes (MBHs) in \Rom{} is largely responsible for the quenched, isolated dwarfs, while isolated dwarfs without an MBH are consistent with quiescent fractions observed in the field. Quenching occurs between $z=0.5-1$, during which the available supply of star-forming gas is heated or evacuated by MBH feedback. Mergers or interactions seem to play little to no role in triggering the MBH feedback. At low stellar masses, $M_{\rm star} \lesssim 10^{9.3} M_\odot$, quenching proceeds across several Gyr as the MBH slowly heats up gas in the central regions. At higher stellar masses, $M_{\rm star} \gtrsim 10^{9.3} M_\odot$, quenching occurs rapidly within $1$ Gyr, with the MBH evacuating gas from the central few kpc of the galaxy and driving it to the outskirts of the halo. Our results indicate the possibility of substantial star formation suppression via MBH feedback within dwarf galaxies in the field. On the other hand, the apparent over-quenching of dwarf galaxies due to MBH suggests higher resolution and/or better modeling is required for MBHs in dwarfs, and quenched fractions offer the opportunity to constrain current models.
